Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...514a..34l&link_type=abstract
Astronomy and Astrophysics, Volume 514, id.A34
Astronomy and Astrophysics
Astrophysics
3
Stars: Early-Type, Binaries: General, Stars: Individual: &Theta, 1 Ori C, Binaries: Spectroscopic, Binaries: Visual
Scientific paper
Context. As the brightest star in the Trapezium cluster, Θ1 Ori C is the youngest and nearest to us among O-stars. It is considered to be a multiple system where the main component is an oblique magnetic rotator. Aims: Here, we aim at explaining the structure of the Θ1 Ori C system. We check for a new hypothesis about the presence of a third component and try to derive the corresponding orbital solutions and the absolute masses of the components. Methods: We measured new radial velocities (RVs) of Θ1 Ori C and and combined them with data from literature. For the analysis, we used multiple frequency search and iterative calculations of orbits based on the method of differential corrections, applying successive prewhitening to the data in both methods. Results are compared with those obtained from speckle observations. Results: We detected the impact of the known distant companion in the RVs of the primary and can now calculate a spectroscopic orbital solution that is consistent with the observed astrometric positions. We find evidence that Θ1 Ori C is at least a triple system consisting of the primary, the known astrometric companion in a wide eccentric orbit with a period of 11 yr, and a second companion in a close eccentric orbit with a period of 61.5 °. We assign the additionally found period of 15.4° d to the rotation of the primary, which is in a 1:4 resonance with the close orbit. Derived masses are 31 Msun for the primary, 12 Msun for the distant, and 1 Msun for the close companion.
Bychkov Victor
Bychkova L.
Klochkova Valentina
Lehmann Holger
Vitrichenko E.
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